Since the discovery of cosmic acceleration ([1]}, [2]}), Type Ia supernova (SN Ia) distance measurements continue to be a critical analysis tool for measuring cosmic distances and the properties of dark energy. To measure the dark energy equation of state, \(w\) , with high precision, accurate SN Ia photometry and calibration is crucial. Efforts to improve these measurements have been made by large-area surveys such as the Sloan Digital Sky Survey (SDSS; [3]}), Supernova Legacy Survey, (SNLS; [4]}, [5]}), Pan-STARRS (PS1; [6]}, [7]}), Dark Energy Survey (DES; [8]}), and Joint Light-curve Analysis (JLA; [9]}). These analyses find that cosmic acceleration is consistent with a cosmological constant (\(w = -1\) ), and the combined statistical and systematic uncertainty on \(w\)  is \(\sim \) 0.05. As part of these measurements, it is important to quantify systematic uncertainties from many effects including zero-points, filter transmissions, and spectral energy distribution (SED) dependencies. Here we explore a new systematic effect related to the local surface brightness (SB) of the underlying galaxy.
